In [1]:
from herschelhelp_internal import git_version
print("This notebook was run with herschelhelp_internal version: \n{}".format(git_version()))
In [2]:
%matplotlib inline
#%config InlineBackend.figure_format = 'svg'
import matplotlib.pyplot as plt
plt.rc('figure', figsize=(10, 6))
import locale
locale.setlocale(locale.LC_ALL, 'en_GB')
import os
import time
import itertools
from astropy.coordinates import SkyCoord
from astropy.table import Table
from astropy import units as u
import numpy as np
from matplotlib_venn import venn3
from herschelhelp_internal.masterlist import nb_compare_mags
In [3]:
OUT_DIR = os.environ.get('OUT_DIR', "./data")
SUFFIX = os.environ.get('SUFFIX', time.strftime("_%Y%m%d"))
master_catalogue = Table.read("{}/master_catalogue_elais-n1{}.fits".format(OUT_DIR, SUFFIX))
I - Summary of wavelength domains¶
In [4]:
flag_obs = master_catalogue['flag_optnir_obs']
flag_det = master_catalogue['flag_optnir_det']
In [5]:
venn3(
[
np.sum(flag_obs == 4),
np.sum(flag_obs == 2),
np.sum(flag_obs == 6),
np.sum(flag_obs == 1),
np.sum(flag_obs == 5),
np.sum(flag_obs == 3),
np.sum(flag_obs == 7)
],
set_labels=('Optical', 'near-IR', 'mid-IR'),
subset_label_formatter=lambda x: "{}%".format(int(100*x/len(flag_obs)))
)
plt.title("Wavelength domain observations");
In [6]:
venn3(
[
np.sum(flag_det[flag_obs == 7] == 4),
np.sum(flag_det[flag_obs == 7] == 2),
np.sum(flag_det[flag_obs == 7] == 6),
np.sum(flag_det[flag_obs == 7] == 1),
np.sum(flag_det[flag_obs == 7] == 5),
np.sum(flag_det[flag_obs == 7] == 3),
np.sum(flag_det[flag_obs == 7] == 7)
],
set_labels=('mid-IR', 'near-IR', 'Optical'),
subset_label_formatter=lambda x: "{}%".format(int(100*x/np.sum(flag_det != 0)))
)
plt.title("Detection of the {} sources detected\n in any wavelength domains "
"(among {} sources)".format(
locale.format('%d', np.sum(flag_det != 0), grouping=True),
locale.format('%d', len(flag_det), grouping=True)));
II - Comparing magnitudes in similar filters¶
The master list if composed of several catalogues containing magnitudes in similar filters on different instruments. We are comparing the magnitudes in these corresponding filters.
In [7]:
u_bands = ["WFC u", "CFHT Megacam u"]
g_bands = ["WFC g", "CFHT Megacam g", "SUPRIME g", "GPC1 g"]
r_bands = ["WFC r", "CFHT Megacam r", "SUPRIME r", "GPC1 r"]
i_bands = ["WFC i", "SUPRIME i", "GPC1 i"]
z_bands = ["WFC z", "CFHT Megacam z", "SUPRIME z", "GPC1 z"]
y_bands = ["SUPRIME y", "GPC1 y"]
In [8]:
for band_of_a_kind in [u_bands, g_bands, r_bands, i_bands, z_bands, y_bands]:
for band1, band2 in itertools.combinations(band_of_a_kind, 2):
basecol1, basecol2 = band1.replace(" ", "_").lower(), band2.replace(" ", "_").lower()
col1, col2 = "m_ap_{}".format(basecol1), "m_ap_{}".format(basecol2)
nb_compare_mags(master_catalogue[col1], master_catalogue[col2],
labels=("{} (aperture)".format(band1), "{} (aperture)".format(band2)))
col1, col2 = "m_{}".format(basecol1), "m_{}".format(basecol2)
nb_compare_mags(master_catalogue[col1], master_catalogue[col2],
labels=("{} (total)".format(band1), "{} (total)".format(band2)))
III - Comparing magnitudes to reference bands¶
Cross-match the master list to SDSS and 2MASS to compare its magnitudes to SDSS and 2MASS ones.
In [9]:
master_catalogue_coords = SkyCoord(master_catalogue['ra'], master_catalogue['dec'])
III.a - Comparing u, g, r, i, and z bands to SDSS¶
The catalogue is cross-matched to SDSS-DR13 withing 0.2 arcsecond.
We compare the u, g, r, i, and z magnitudes to those from SDSS using fiberMag for the aperture magnitude and petroMag for the total magnitude.
In [10]:
sdss = Table.read("../../dmu0/dmu0_SDSS-DR13/data/SDSS-DR13_ELAIS-N1.fits")
sdss_coords = SkyCoord(sdss['ra'] * u.deg, sdss['dec'] * u.deg)
idx, d2d, _ = sdss_coords.match_to_catalog_sky(master_catalogue_coords)
mask = (d2d < 0.2 * u.arcsec)
sdss = sdss[mask]
ml_sdss_idx = idx[mask]
In [11]:
for band_of_a_kind in [u_bands, g_bands, r_bands, i_bands, z_bands]:
for band in band_of_a_kind:
sdss_mag_ap = sdss["fiberMag_{}".format(band[-1])]
master_cat_mag_ap = master_catalogue["m_ap_{}".format(band.replace(" ", "_").lower())][ml_sdss_idx]
nb_compare_mags(sdss_mag_ap, master_cat_mag_ap,
labels=("SDSS {} (fiberMag)".format(band[-1]), "{} (aperture)".format(band)))
sdss_mag_tot = sdss["petroMag_{}".format(band[-1])]
master_cat_mag_tot = master_catalogue["m_ap_{}".format(band.replace(" ", "_").lower())][ml_sdss_idx]
nb_compare_mags(sdss_mag_ap, master_cat_mag_ap,
labels=("SDSS {} (petroMag)".format(band[-1]), "{} (total)".format(band)))
III.b - Comparing J and K bands to 2MASS¶
The catalogue is cross-matched to 2MASS-PSC withing 0.2 arcsecond.
We compare the UKIDSS total J and K magnitudes to those from 2MASS.
In [12]:
twomass = Table.read("../../dmu0/dmu0_2MASS-point-sources/data/2MASS-PSC_ELAIS-N1.fits")
twomass_coords = SkyCoord(twomass['raj2000'], twomass['dej2000'])
idx, d2d, _ = twomass_coords.match_to_catalog_sky(master_catalogue_coords)
mask = (d2d < 0.2 * u.arcsec)
twomass = twomass[mask]
ml_twomass_idx = idx[mask]
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nb_compare_mags(twomass['jmag'], master_catalogue['m_ukidss_j'][ml_twomass_idx],
labels=("2MASS J", "UKIDSS J (total)"))
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nb_compare_mags(twomass['kmag'], master_catalogue['m_ukidss_k'][ml_twomass_idx],
labels=("2MASS K", "UKIDSS K (total)"))
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